We propose to obtain low-resolution full-scan SWS01 spectra and PHT03
25, 60 and 100 micron data for a sample of 15 supergiants (SGs) in the
Magellanic Clouds (the Clouds) which have a large infrared excess. ISO
is the only platform with the spectroscopic capability and sensitivity
to observe stars over a wide wavelength range in galaxies other than
our own.

We will derive properties of the stellar and circumstellar environment
of individual SGs in the Clouds, in particular the mass loss rate
(history), luminosity, intrinsic shape of the silicate 9.8 and 18 micron
dust features and the effective temperature. This will be achieved
by fitting the data with a radiative transfer model and follow-up
ground-based observations.

The results will be compared to that of similar observations of SGs in
the Galaxy obtained in the Central Program by TDEJONG_AGBSTARS.  This
will provide information on the metallicity dependence of the mass
loss rate, which is essentially not known at the moment, but is of key
importance for the theory of dust driven stellar winds and for massive
star evolution.

With the luminosity, effective temperature AND the mass loss rate of
individual SGs known, the observations will be compared to, and
constrain, evolutionary models of massive stars. This will lead to a
better understanding of the post-main sequence evolution of massive
stars in general, and the relative importance of blue --> red and
red --> blue evolution, the pre-supernova progenitor type distribution,
and the importance of the post-RSG channel for Wolf-Rayet star
formation in particular.